The University of Southampton
University of Southampton Institutional Repository

PSR J0030+0451 mass and radius from NICER data and implications for the properties of neutron star matter

PSR J0030+0451 mass and radius from NICER data and implications for the properties of neutron star matter
PSR J0030+0451 mass and radius from NICER data and implications for the properties of neutron star matter
Neutron stars are not only of astrophysical interest, but are also of great interest to nuclear physicists because their attributes can be used to determine the properties of the dense matter in their cores. One of the most informative approaches for determining the equation of state (EoS) of this dense matter is to measure both a star's equatorial circumferential radius R e and its gravitational mass M. Here we report estimates of the mass and radius of the isolated 205.53 Hz millisecond pulsar PSR J0030+0451 obtained using a Bayesian inference approach to analyze its energy-dependent thermal X-ray waveform, which was observed using the Neutron Star Interior Composition Explorer (NICER). This approach is thought to be less subject to systematic errors than other approaches for estimating neutron star radii. We explored a variety of emission patterns on the stellar surface. Our best-fit model has three oval, uniform-temperature emitting spots and provides an excellent description of the pulse waveform observed using NICER. The radius and mass estimates given by this model are ${R}_{e}={13.02}_{-1.06}^{+1.24}$ km and $M={1.44}_{-0.14}^{+0.15}\,{M}_{\odot }$ (68%). The independent analysis reported in the companion paper by Riley et al. explores different emitting spot models, but finds spot shapes and locations and estimates of R e and M that are consistent with those found in this work. We show that our measurements of R e and M for PSR J0030+0451 improve the astrophysical constraints on the EoS of cold, catalyzed matter above nuclear saturation density.
2041-8205
Miller, Cole
53a83c59-490d-4a67-812c-12b65429ed1a
Lamb, Frederick K.
9e159a6c-8526-41e9-ada4-c8c36ff1bead
Dittmann, A. J.
056e8fde-c082-4555-854a-54004f1d33e6
Bogdanov, Slavko
39f20582-4d71-4b1a-ae2a-b266367341ef
Arzoumanian, Zaven
5befbba6-f6a1-47c8-ae9e-021c5d854a64
Gendreau, Keith C.
cad26609-b22d-4c1d-ada3-4af51e2cd780
Harding, Alice K.
8343154a-9dbd-4454-ae91-feca27dff912
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Lattimer, James M.
443276d9-5096-488e-998e-b7160083cfdc
Ludlam, Renee M.
b27b6ff8-9743-49f2-833a-115803efa43a
Mahmoodifar, Simin
8c38d862-86dd-428d-a5ff-2cdc7bbfc223
Morsink, Sharon
b5dbdf8d-5563-4368-90da-3500e6de0fd5
Ray, Paul S.
773c1940-2b53-4871-8176-c363521bb83f
Riley, Thomas E.
fb72d2bc-54e5-4cbd-a3ee-93b0954e8ad3
Wood, Kent S.
1a18d32c-94a8-427d-b9a6-84282eb53c9d
Enoto, T.
c5c94b63-52c8-4fd2-bd9e-260a84fff52c
Foster, R.
7824f3f8-0a23-425b-bddb-3c794c09cb5d
Okajima, T.
580cfa03-aaa3-4acb-9bd6-8ec6d617f63e
Prigozhin, Gregory Y.
2ddfd21c-ec49-4ba1-a830-d9f7de3d79ad
Soong, Y.
d0102daa-8df7-4c51-97aa-75d7ec3f4913
Miller, Cole
53a83c59-490d-4a67-812c-12b65429ed1a
Lamb, Frederick K.
9e159a6c-8526-41e9-ada4-c8c36ff1bead
Dittmann, A. J.
056e8fde-c082-4555-854a-54004f1d33e6
Bogdanov, Slavko
39f20582-4d71-4b1a-ae2a-b266367341ef
Arzoumanian, Zaven
5befbba6-f6a1-47c8-ae9e-021c5d854a64
Gendreau, Keith C.
cad26609-b22d-4c1d-ada3-4af51e2cd780
Harding, Alice K.
8343154a-9dbd-4454-ae91-feca27dff912
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Lattimer, James M.
443276d9-5096-488e-998e-b7160083cfdc
Ludlam, Renee M.
b27b6ff8-9743-49f2-833a-115803efa43a
Mahmoodifar, Simin
8c38d862-86dd-428d-a5ff-2cdc7bbfc223
Morsink, Sharon
b5dbdf8d-5563-4368-90da-3500e6de0fd5
Ray, Paul S.
773c1940-2b53-4871-8176-c363521bb83f
Riley, Thomas E.
fb72d2bc-54e5-4cbd-a3ee-93b0954e8ad3
Wood, Kent S.
1a18d32c-94a8-427d-b9a6-84282eb53c9d
Enoto, T.
c5c94b63-52c8-4fd2-bd9e-260a84fff52c
Foster, R.
7824f3f8-0a23-425b-bddb-3c794c09cb5d
Okajima, T.
580cfa03-aaa3-4acb-9bd6-8ec6d617f63e
Prigozhin, Gregory Y.
2ddfd21c-ec49-4ba1-a830-d9f7de3d79ad
Soong, Y.
d0102daa-8df7-4c51-97aa-75d7ec3f4913

Miller, Cole, Lamb, Frederick K., Dittmann, A. J., Bogdanov, Slavko, Arzoumanian, Zaven, Gendreau, Keith C., Harding, Alice K., Ho, Wynn C.G., Lattimer, James M., Ludlam, Renee M., Mahmoodifar, Simin, Morsink, Sharon, Ray, Paul S., Riley, Thomas E., Wood, Kent S., Enoto, T., Foster, R., Okajima, T., Prigozhin, Gregory Y. and Soong, Y. (2019) PSR J0030+0451 mass and radius from NICER data and implications for the properties of neutron star matter. Astrophysical Journal Letters, 887 (1), [L24]. (doi:10.3847/2041-8213/ab50c5).

Record type: Article

Abstract

Neutron stars are not only of astrophysical interest, but are also of great interest to nuclear physicists because their attributes can be used to determine the properties of the dense matter in their cores. One of the most informative approaches for determining the equation of state (EoS) of this dense matter is to measure both a star's equatorial circumferential radius R e and its gravitational mass M. Here we report estimates of the mass and radius of the isolated 205.53 Hz millisecond pulsar PSR J0030+0451 obtained using a Bayesian inference approach to analyze its energy-dependent thermal X-ray waveform, which was observed using the Neutron Star Interior Composition Explorer (NICER). This approach is thought to be less subject to systematic errors than other approaches for estimating neutron star radii. We explored a variety of emission patterns on the stellar surface. Our best-fit model has three oval, uniform-temperature emitting spots and provides an excellent description of the pulse waveform observed using NICER. The radius and mass estimates given by this model are ${R}_{e}={13.02}_{-1.06}^{+1.24}$ km and $M={1.44}_{-0.14}^{+0.15}\,{M}_{\odot }$ (68%). The independent analysis reported in the companion paper by Riley et al. explores different emitting spot models, but finds spot shapes and locations and estimates of R e and M that are consistent with those found in this work. We show that our measurements of R e and M for PSR J0030+0451 improve the astrophysical constraints on the EoS of cold, catalyzed matter above nuclear saturation density.

Text
1912.05705 - Accepted Manuscript
Download (21MB)

More information

Accepted/In Press date: 24 October 2019
Published date: 12 December 2019

Identifiers

Local EPrints ID: 436752
URI: http://eprints.soton.ac.uk/id/eprint/436752
ISSN: 2041-8205
PURE UUID: 39419cff-4777-449c-8495-a38cc4a5ec7d
ORCID for Wynn C.G. Ho: ORCID iD orcid.org/0000-0002-6089-6836

Catalogue record

Date deposited: 03 Jan 2020 17:30
Last modified: 05 Feb 2020 01:30

Export record

Altmetrics

Contributors

Author: Cole Miller
Author: Frederick K. Lamb
Author: A. J. Dittmann
Author: Slavko Bogdanov
Author: Zaven Arzoumanian
Author: Keith C. Gendreau
Author: Alice K. Harding
Author: Wynn C.G. Ho ORCID iD
Author: James M. Lattimer
Author: Renee M. Ludlam
Author: Simin Mahmoodifar
Author: Sharon Morsink
Author: Paul S. Ray
Author: Thomas E. Riley
Author: Kent S. Wood
Author: T. Enoto
Author: R. Foster
Author: T. Okajima
Author: Gregory Y. Prigozhin
Author: Y. Soong

University divisions

Download statistics

Downloads from ePrints over the past year. Other digital versions may also be available to download e.g. from the publisher's website.

View more statistics

Atom RSS 1.0 RSS 2.0

Contact ePrints Soton: eprints@soton.ac.uk

ePrints Soton supports OAI 2.0 with a base URL of http://eprints.soton.ac.uk/cgi/oai2

This repository has been built using EPrints software, developed at the University of Southampton, but available to everyone to use.

We use cookies to ensure that we give you the best experience on our website. If you continue without changing your settings, we will assume that you are happy to receive cookies on the University of Southampton website.

×